A proper motion study of the globular cluster M12 (NGC 6218)

Sariya, Devesh P.; Jiang, Ing-Guey; Yadav, R. K. S.

doi:10.1088/1674-4527/18/10/126

Cited by 8 publications

(3 citation statements)

References 52 publications

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“…We used the method presented by Balaguer-Núñez et al (1998) to determined the membership probabilities. This method was previously used for open and globular clusters (Sariya et al 2018(Sariya et al , 2021aBisht et al 2020Bisht et al , 2021Bisht et al , 2022. Sariya et al (2018) give a detailed description of this method.…”

Section: Membership Probabilitiesmentioning

confidence: 99%

A Gaia based analysis of open cluster Berkeley 27

et al. 2023

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Section: Membership Probabilitiesmentioning

confidence: 99%

A Gaia based analysis of open cluster Berkeley 27

et al. 2023

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“…A circle of 0.3, 0.6, 0.4, 0.4, and 0.3 mas yr −1 for clusters Pi 2, Pi 3, Pi 7, Pi 12, and Pi 15, respectively, around the distribution of cluster stars in the VPDs, characterizes our membership criteria. The selected radius in VPDs compromises losing cluster members with poor PMs and including field region stars (Sariya et al 2018). The cluster's member stars are gravitationally bound, so they show a very narrow spread in parallaxes compared to field stars in parallax versus magnitude plots (Angelo et al 2020).…”

Section: Mean Proper Motion and Field Star Separationmentioning

confidence: 99%

“…It is required to separate field stars from the cluster member stars to estimate the physical and dynamical parameters of the clusters (e.g., Dias et al 2018aDias et al , 2018bSariya et al 2018;Bisht et al 2021b;Sariya et al 2021;Bisht et al 2021aBisht et al , 2022. We have adopted the approach given by Balaguer-Núñez et al (1998) by using the PM database from the Gaia EDR3 catalog to determine the membership of stars in Pismis clusters.…”

Section: Membership Probabilitiesmentioning

confidence: 99%

A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3

Bisht

Zhu

Elsanhoury

et al. 2022

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Open clusters are groups of stars that form simultaneously; hence, these are excellent probes to test theories of star formation, stellar evolution, and dynamics in the Milky Way disk. We carry out a detailed photometric and kinematic study of five poorly studied intermediate-age open clusters, Pismis 2 (Pi 2), Pismis 3 (Pi 3), Pismis 7 (Pi 7), Pismis 12 (Pi 12), and Pismis 15 (Pi 15), using the Gaia EDR3 database. By estimating the membership probabilities of stars, we recognized 635, 1488, 535, 368, and 494 most probable members for these clusters by using proper-motion and parallax data taken from Gaia EDR3. The radial density profiles of cluster members provide cluster radii of 4.′5–6.′5 for these clusters. Their ages range from 0.9 to 2.5 Gyr, and distances range, using parallax, from 2.15 to 5.10 kpc. The overall mass function slopes for main-sequence stars are found as 0.27 ± 0.16 (for 1.0–1.6 M ⊙ stars), 0.86 ± 0.27 (for 1.0–2.1 M ⊙ stars), 1.08 ± 0.32 (for 1.0–2.2 M ⊙ stars), 0.89 ± 0.38 (for 1.0–2.2 M ⊙ stars), and 1.07 ± 0.28 (for 1.0–2.1 M ⊙ stars) for clusters Pi 2, Pi 3, Pi 7, Pi 12, and Pi 15. Our obtained values of slopes are flatter in comparison with Salpeter’s value (x = 1.35) within uncertainty. The present study demonstrates that all these Pismis clusters are dynamically relaxed. We found that these objects follow a circular path around the Galactic center. We compute these clusters’ apex coordinates (A, D) and other kinematic parameters.

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An Investigation of Poorly Studied Open Cluster NGC 4337 Using Multicolor Photometric and Gaia DR2 Astrometric Data

Bisht

Elsanhoury

Zhu

et al. 2020

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We present a comprehensive analysis (photometric and kinematical) of the poorly studied open cluster NGC 4337 using 2MASS, WISE, APASS, and Gaia DR2 databases. By determining the membership probabilities of stars, we identified the 624 most probable members with membership probability higher than 50% by using proper motion and parallax data taken from Gaia DR2. The mean proper motion of the cluster is obtained as and μ y = 1.49 ± 0.006 mas yr−1. We find the normal interstellar extinction toward the cluster region. The radial distribution of members provides a cluster radius of 7.′75 (5.63 pc). The estimated age of 1600 ± 180 Myr indicates that NGC 4337 is an old open cluster with a bunch of red giant stars. The overall mass function slope for main-sequence stars is found as within the mass range 0.75−2.0 , which is in fair agreement with Salpeter’s value (x = 1.35) within uncertainty. The present study demonstrates that NGC 4337 is a dynamically relaxed open cluster. Using the Galactic potential model, Galactic orbits are obtained for NGC 4337. We found that this object follows a circular path around the Galactic center. Under the kinematical analysis, we compute the apex coordinates (A, D) by using two methods: (i) the classical convergent point method and (ii) the AD-diagram method. The obtained coordinates are (A conv, D conv) = (96.°27 ± 0.°10, 13.°14 ± 0.°27) and (A ◦, D ◦) = (100.°282 ± 0.°10, 9.°577 ± 0.°323) respectively. We also computed the Velocity Ellipsoid Parameters, matrix elements (μ ij ), direction cosines (l j , m j , n j ), and the Galactic longitude of the vertex (l 2).

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A proper motion study of the globular cluster M12 (NGC 6218)

Cited by 8 publications

References 52 publications

A Gaia based analysis of open cluster Berkeley 27

A Gaia based analysis of open cluster Berkeley 27

A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3

An Investigation of Poorly Studied Open Cluster NGC 4337 Using Multicolor Photometric and Gaia DR2 Astrometric Data

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